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QUIET Summary. Probing Inflationary Scalar fields at GUT-scale energies Phase I has already demonstrated its technology and methodology (100 detectors) The most sensitive CMB polarization array yet fielded Phase II has been proposed NSF Reverse site visit in Jan-Feb

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quiet summary
QUIET Summary
  • Probing Inflationary Scalar fields at GUT-scale energies
  • Phase I has already demonstrated its technology and methodology (100 detectors)
    • The most sensitive CMB polarization array yet fielded
  • Phase II has been proposed
    • NSF Reverse site visit in Jan-Feb
    • FNAL involvement critical to get to Phase II level (1600)
      • “HEP” approach more important as experiments grow
  • QUIET is unique: (verified) technology, frequencies, year-round access, best able to forecast sensitivity, and alliances with other experiments
  • The Cosmic Microwave Background and Particle Physics
  • M. Kamionkowski, A. Kosowsky, Ann.Rev.Nucl.Part.Sci.49:77-123,1999
  • The Cosmic Microwave Background for Pedestrians: A Review for Particle and Nuclear Physicists
  • D. Samtleben, S. Staggs, B. W., Ann.Rev.Nucl.Part.Sci.57:245-283,2007
slide2
Manchester

Oxford

Chicago (KICP)

Fermilab

Oslo

MPI-Bonn

Stanford

(KIPAC)

KEK

Caltech

JPL

Columbia

Princeton

Miami

Chajnantor Plateau, Chile

FNAL PAC

2

the site atacama desert in chile
The Site: Atacama Desert in Chile
  • Home for many expts
    • ALMA, ACT, ASTE, QUIET, POLARBEAR, CLOVER, …
  • High and Dry:
    • 16,700 feet
  • Year-round access
  • Lots of room

FNAL PAC

integrating the w band array the chicago
Integrating the W-band Array the Chicago

(5 times as many elements to be integrated at FNAL)

FNAL PAC

slide6
Ey

Ea

Eb

Ex

4kHz phase switching

Q

U

QUIET L/R Correlator:

Simultaneous Q/U measurements

FNAL PAC

An Unpolarized pixel gives ZERO even with a gain difference between the legs!

8 sec of data 100khz sampling
8 sec of data 100kHz sampling

Temperature vs. time, 10 ms bins

unswitched

switched

FNAL PAC

slide8
Map precision on

1x1 degree pixel:

Planck: 1 K (100 GHz)

QUIET: 10-1K (90 GHz)

FNAL PAC

slide9
Q

U

Galaxy

(Pol., <100 hrs)

sytematicefects

not considered yet

WMAP

5 years

FNAL PAC

slide11
QUIET ~ 600 hrs WMAP 5 years

QUIET-I Stokes Q map of one patch:

Already deeper than Planck forecasts

FNAL PAC

phase i has already shown
Phase I has already shown:
  • Platelet, OMT technology works
  • Module technology works
    • Want to improve sensitivity and production
  • Crossed Dragone Optics verified
    • Now the most popular choice
  • High speed sampling works and is valuable
  • The site works: duty cycle, atmosphere
  • We can reliable forecast Phase II
  • Cautious approach has paid off

FNAL PAC

phase ii plan
Phase II Plan
  • 4 Telescopes
    • (3 CMB & 1 Foreground)
  • “Small things”
    • Electronics improvements
    • Thermal control
    • Matching band-passes
  • “Big things”
    • Improving module production
    • Improving module performance

FNAL PAC

foregrounds planck sky model
QUIET

Polarbear

ABS, SPT

Foregrounds(Planck Sky Model)
  • Dust(synchrotron) negligible for QUIET(SPT)
  • Broad frequency range important to determine contamination
  • 100% overlap with ABS, Polarbear; less w/SPT

r=0.1

FNAL PAC

slide17
Current* Performance

(noise, duty cycle, 1/f)

Likely Improvements

0.018r0.005



FNAL PAC

< 0.3 ev

10lensing35

* already better!

slide18
“While QUIET I has been pursued primarily with non-HEP funding, HEP has unique capabilities to offer the project as it moves to the next step, QUIET II: (a) Fermilab has unique large-scale fabrication capabilities required to mass-produce the detectors; (b) HEP scientists have valuable experience with the high-speed electronics the project will require; (c) the approaches to data analysis and related capabilities that have been developed for particle physics experiments will become increasingly important to CMB science as the scope of CMB experiments, and scale of the collaborations, increases.
  • Recommendations: PASAG recommends that QUIET II be supported at the proposed scope under all budget scenarios. Given the central importance of the CMB to our understanding of energy, matter, space, and time and the unique contributions HEP can provide to CMB science, PASAG further recommends that the future upgrade path for QUIET II should be considered for support at the appropriate time.”

Field does support multiple efforts, e.g. Dark Matter searches

FNAL PAC

what characterizes distinguishes quiet
What Characterizes/Distinguishes QUIET?
  • Unique RF technology
    • Different systematics, Q & U measured simultaneously
    • Large dynamic range
  • Modulation:
    • 4 kHz inside modules
    • From sky rotation: Q to U to -Q every 6 hours
    • From telescope deck rotation: Q to U every week
  • ~6% of the sky mapped 100 times deeper than Planck
    • Sensitivity to r < 0.02 [based on current performance (noise, duty cycle)]
  • Alliance with (bolometric) POLARBEAR and ABS (and SPT)
    • Identical Patches
    • frequencies straddle WMAP “sweet spot”
  • HEP-like:
    • 800kHz digitization (FPGA demodulation)
    • Volume production, quality control
    • simulations, data reduction, blind analyses, systematics, systematics, …..
    • Increased appreciation of our field
  • Upgrade Path:
    • Sharing ATACAMA telescopes
    • MMIC improvements: from 15 QL to 8 QL to 3QL

FNAL PAC

atacama experiments
ATACAMA Experiments

32/

NSF Site Visit – May 18 - 19, 2009

NSF Site Visit – May 18 - 19, 2009

current cmb polarization status
Current CMB Polarization Status

(QUIET has already collected data which will improve these measurements)

FNAL PAC

telescope
Telescope
  • 1.4m primary mirror
  • FWHM:
    • 13 arcmin (W-band)
    • 28 arcmin (Q-band)

FNAL PAC

slide26
+Q

-Q

+Q

-Q

High Speed Sampling18 bits @ 800 kHz

Q/U measurement every 250 s

Monitors high-frequency noise

Permits Quadrature Samples

  • TOD noise with no signal

0.5ms

FNAL PAC

slide27
Moon

PRELIMINARY

WMAP

Galaxy

(TT, <100 hrs)

QUIET

FNAL PAC

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